I present the validation and characterization of Kepler-410. Despite its brightness (V = 9.4) and its identification as a planetary candidate at the beginning of the Kepler mission, this system still awaited its confirmation. This is because of the small (2.8 Rearth) and presumably low-mass planet candidate, its long orbit (P = 17.8 days), and the presence of a second star in the system. The system also shows transit timing variations.

Using asteroseismology as well as a variety of data from space and ground based observatories, we were able to confirm the planetary nature of the system. We further determined a number of system properties, including the stellar inclination and planetary eccentricity. Both of these parameters could only be determined through the use of asteroseismology. Kepler-410 has an inclination of 82.5 [+7.5, -2.5] degrees indicative of a low stellar obliquity, and a non-circular orbit with an eccentricity of 0.17+-0.07. I will close the talk by presenting new asteroseismic eccentricity determinations in other multi-planet systems harboring low mass planets.